The most metal-poor galaxies
... 1 Introduction – What is a metal-poor galaxy? The discovery of extragalactic objects with very low heavy element abundance was made by Searle and Sargent (1972) who reported on the properties of two intriguing galaxies, IZw18 and IIZw40. They emphasised that they could be genuinely young galaxies i ...
... 1 Introduction – What is a metal-poor galaxy? The discovery of extragalactic objects with very low heavy element abundance was made by Searle and Sargent (1972) who reported on the properties of two intriguing galaxies, IZw18 and IIZw40. They emphasised that they could be genuinely young galaxies i ...
Teaching Tips Table of Contents - Hubble Deep Field
... The Mathematical World: C. Shapes By the end of 8th grade, students should know that ...
... The Mathematical World: C. Shapes By the end of 8th grade, students should know that ...
13_InstructorSolutions
... EVALUATE: The amplitude and the maximum speed depend on the total energy of the system but the angular frequency is independent of the amount of energy in the system and just depends on the force constant of the spring and the mass of the object. IDENTIFY: K = 12 mv 2 , U grav = mgy and U el = 12 kx ...
... EVALUATE: The amplitude and the maximum speed depend on the total energy of the system but the angular frequency is independent of the amount of energy in the system and just depends on the force constant of the spring and the mass of the object. IDENTIFY: K = 12 mv 2 , U grav = mgy and U el = 12 kx ...
Article PDF - IOPscience
... In Section 2, we describe the CSO sample and the observations taken with Spitzer; we describe the data reduction process in Section 3. Section 4 presents results of the observations, including full spectra and data tables for all measured features. We derive physical properties for the CSO hosts in ...
... In Section 2, we describe the CSO sample and the observations taken with Spitzer; we describe the data reduction process in Section 3. Section 4 presents results of the observations, including full spectra and data tables for all measured features. We derive physical properties for the CSO hosts in ...
Realizing nonholonomic dynamics as limit of friction forces
... mechanics can be viewed as letting the mass in the mechanical metric go to infinity along constrained directions [Koz83]. See also [Koz92] for a discussion of various methods to realize constraints in dynamics and [BKM+ 15, Sec. 0.3] for a review of the applicability of nonholonomic dynamics to slid ...
... mechanics can be viewed as letting the mass in the mechanical metric go to infinity along constrained directions [Koz83]. See also [Koz92] for a discussion of various methods to realize constraints in dynamics and [BKM+ 15, Sec. 0.3] for a review of the applicability of nonholonomic dynamics to slid ...
EROs and submm galaxies: Expectations for FMOS in the
... been resolved into submillimetre galaxies (SMGs) which appear to be dusty vigorous star-forming galaxies. Half the total extragalactic background is in the submm, while SMGs make up more than half the extragalactic submm background >25% of all stars since the Big Bang have formed in SMGs. ...
... been resolved into submillimetre galaxies (SMGs) which appear to be dusty vigorous star-forming galaxies. Half the total extragalactic background is in the submm, while SMGs make up more than half the extragalactic submm background >25% of all stars since the Big Bang have formed in SMGs. ...
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... roughly 73% of the total. The total energy density adds up to a “critical density” which suggests that the universe is geometrically flat (as discussed below). This combination of theory and observations forms the entire theoretical basis of Big Bang cosmology, and produces very specific prediction ...
... roughly 73% of the total. The total energy density adds up to a “critical density” which suggests that the universe is geometrically flat (as discussed below). This combination of theory and observations forms the entire theoretical basis of Big Bang cosmology, and produces very specific prediction ...
The correlation between galaxy morphology and star
... panchromatic catalog of the GOODS–South field (see also Guo et al. 2011, 2012, where key results and features of the SED fitting have been discussed). Prior to carrying out the SED fitting, photometric redshifts have been measured for all galaxies from the 13–band UBVizYJHKsI1 I2 I3 I4 photometry us ...
... panchromatic catalog of the GOODS–South field (see also Guo et al. 2011, 2012, where key results and features of the SED fitting have been discussed). Prior to carrying out the SED fitting, photometric redshifts have been measured for all galaxies from the 13–band UBVizYJHKsI1 I2 I3 I4 photometry us ...
1 Globular Cluster Systems - McMaster Physics and Astronomy
... these heavily reddened clusters remained surprisingly poor, and even today there are still a few clusters with exceptionally high reddenings embedded deep in the Galactic bulge about which we know almost nothing (see the listings in Harris 1996a). However, progress over the years has been steady and ...
... these heavily reddened clusters remained surprisingly poor, and even today there are still a few clusters with exceptionally high reddenings embedded deep in the Galactic bulge about which we know almost nothing (see the listings in Harris 1996a). However, progress over the years has been steady and ...
The Life Cycle of Stars: Supernovae in Starbursts by Jason Kezwer
... extinction. Interpreting this as a supernova-related event we estimate the extinction in the nuclear regions of Arp 220 to lie between 2.01 ≤ AK ≤ 3.40 or 17.95 ≤ AV ≤ 30.36 in the optical, in agreement with several other estimates. Improved resolution is required in order to detect supernovae in th ...
... extinction. Interpreting this as a supernova-related event we estimate the extinction in the nuclear regions of Arp 220 to lie between 2.01 ≤ AK ≤ 3.40 or 17.95 ≤ AV ≤ 30.36 in the optical, in agreement with several other estimates. Improved resolution is required in order to detect supernovae in th ...
A Universal Stellar Initial Mass Function? A Critical Look Further
... Way! Elmegreen & Scalo (2006) provide a detailed exploration of the degeneracies involved in inferring a stellar population’s IMF from its measured PDMF and adopted SFH. It is somewhat disconcerting that the break from the Salpeter law identified in many IMF studies needs to be invoked near the plac ...
... Way! Elmegreen & Scalo (2006) provide a detailed exploration of the degeneracies involved in inferring a stellar population’s IMF from its measured PDMF and adopted SFH. It is somewhat disconcerting that the break from the Salpeter law identified in many IMF studies needs to be invoked near the plac ...
Modified Newtonian dynamics
In physics, modified Newtonian dynamics (MOND) is a theory that proposes a modification of Newton's laws to account for observed properties of galaxies. Created in 1983 by Israeli physicist Mordehai Milgrom, the theory's original motivation was to explain the fact that the velocities of stars in galaxies were observed to be larger than expected based on Newtonian mechanics. Milgrom noted that this discrepancy could be resolved if the gravitational force experienced by a star in the outer regions of a galaxy was proportional to the square of its centripetal acceleration (as opposed to the centripetal acceleration itself, as in Newton's Second Law), or alternatively if gravitational force came to vary inversely with radius (as opposed to the inverse square of the radius, as in Newton's Law of Gravity). In MOND, violation of Newton's Laws occurs at extremely small accelerations, characteristic of galaxies yet far below anything typically encountered in the Solar System or on Earth.MOND is an example of a class of theories known as modified gravity, and is an alternative to the hypothesis that the dynamics of galaxies are determined by massive, invisible dark matter halos. Since Milgrom's original proposal, MOND has successfully predicted a variety of galactic phenomena that are difficult to understand from a dark matter perspective. However, MOND and its generalisations do not adequately account for observed properties of galaxy clusters, and no satisfactory cosmological model has been constructed from the theory.